From: LARRY KLAES (ljk4_at_msn.com)
Date: Thu Sep 01 2005 - 13:55:15 UTC
Paper: astro-ph/0508678
Date: Wed, 31 Aug 2005 13:10:47 GMT (15kb)
Title: Disks and Planets Around Massive White Dwarfs
Authors: M. Livio (Space Telescope, Univ. of St. Andrews), J. E. Pringle
(Univ.
of St. Andrews, Inst. of Astronomy), K. Wood (Univ. of St. Andrews)
Comments: 8 pages, 1 figure; accepted ApJL
Report-no: ST ScI Eprint #1678
\\
We predict the existence of dusty disks and possibly CO planets around
massive white dwarfs. We show that the thermal emission from these disks
should
be detectable in the infrared. The planets may also be detectable either by
direct IR imaging, spectroscopy, or using the pulsations of the white
dwarfs.
\\ ( http://arXiv.org/abs/astro-ph/0508678 , 15kb)
Paper: astro-ph/0508691
Date: Wed, 31 Aug 2005 18:49:23 GMT (442kb)
Title: Simulating the boundary layer between a white dwarf and its accretion
disc
Authors: Jacob Lund Fisker & Dinshaw S. Balsara
Comments: 8 pages, 2 figures
\\
We describe the results of numerical simulations of the dynamics of the
boundary layer (BL) between the accretion disk and the surface of a
non-magnetic white dwarf (WD) for different viscosities which corresponds to
different stages for dwarf novae burst cycles. The simulations cover the
inner
part of the accretion disk, the BL, and the upper atmosphere of the star.
The
high viscosity case, which corresponds to a dwarf nova in outburst, shows a
optically thick BL which after one Keplerian rotation period ($t_K$=19s)
extends up to 20-25 degrees to either side of the disk plane. The BL is
optically thick and thus occludes part of the star. The low viscosity case,
which corresponds to a dwarf nova in quiescense, also shows a BL, but it is
optically thin.
\\ ( http://arXiv.org/abs/astro-ph/0508691 , 442kb)
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